SIMBAD references

We compare the distribution of H I 21 cm, H II 6563 Å, and [C II] 157.7 µm line emission over the entire Large Magellanic Cloud (LMC). Bright [C II] emission is associated with H II regions and their surroundings, with a good correlation between [C II] and Hα filaments. Faint [C II] emission is also detected in regions with no H II emission. We found a reasonably good correlation between the extended [C II] emission and H I emission. Using the slope of the [C II] versus H I correlation in regions with low Hα brightness, 4πI_CII_/NHI_=6.0±3.0x10^–26 ergs.s^–1 (H atom)^–1, and the total H I column density away from H II regions, the luminosity of [C II] from the atomic medium is 1.14±0.57x10⁶L_☉, which amounts to 20% of the total [C II] luminosity from the LMC. The [C II] emission per unit H I column density from the atomic regions of the LMC is similar to, but somewhat higher than, that in the Milky Way, because of the cancelling effects of lower C abundance and higher radiation field in the LMC. Significant deviations between the H I and [C II] in some regions suggest that part of the [C II] emission comes from ionized regions. Subtracting the contribution to the [C II] luminosity from bright H II regions, an upper limit of 46% of the [C II] luminosity could be due to diffuse ionized gas.